Relativistic Dynamics and Mass Exchange in Binary Black Hole Mini-disks

被引：58

作者：

Bowen, Dennis B. ^{[1
]}

Campanelli, Manuela ^{[1
]}

Krolik, Julian H. ^{[2
]}

Mewes, Vassilios ^{[1
]}

Noble, Scott C. ^{[3
]}

机构：

[1] Rochester Inst Technol, Ctr Computat Relat & Gravitat, Rochester, NY 14623 USA

[2] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA

[3] Univ Tulsa, Dept Phys & Engn Phys, Tulsa, OK 74104 USA

来源：

ASTROPHYSICAL JOURNAL | 2017年 / 838卷 / 01期

基金：

美国国家科学基金会;

关键词：

accretion; accretion disks; black hole physics; galaxies: nuclei; hydrodynamics; ACCRETION DISKS; ANGULAR-MOMENTUM; MAGNETOHYDRODYNAMIC SIMULATIONS; 3-DIMENSIONAL WAVES; DENSITY WAVES; TIDAL TORQUES; MERGERS; INSTABILITIES; RESONANCES; EVOLUTION;

D O I：

10.3847/1538-4357/aa63f3

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present the first exploration of gas dynamics in a relativistic binary black hole (BH) system in which an accretion disk (a "mini-disk") orbits each BH. We focus on 2D hydrodynamical studies of comparable-mass, non-spinning systems. Relativistic effects alter the dynamics of gas in this environment in several ways. Because the gravitational potential between the two BHs becomes shallower than in the Newtonian regime, the mini-disks stretch toward the L1 point and the amount of gas passing back and forth between the mini. disks increases sharply with decreasing binary separation. This "sloshing" is quasi-periodically modulated at 2 and 2.75 times the binary orbital frequency, corresponding to timescales of hours to days for supermassive binary black holes (SMBBHs). In addition, relativistic effects add an m = 1 component to the tidally driven spiral waves in the disks that are purely m = 2 in Newtonian gravity; this component becomes dominant when the separation is less than or similar to 100 gravitational radii. Both the sloshing and the spiral waves have the potential to create distinctive radiation features that may uniquely mark SMBBHs in the relativistic regime.

引用

页数：20

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